The satellites of Saturn were observed with the 60-inch telescope at
Palomar Mountain during the Saturn Ring Plane Crossing (RPX) on August
9-12, 1995. Observations were obtained with a 1024 square CCD and a
methane filter to reduce light from Saturn. During the four nights more
than 250 images were obtained. These images enable a rare opportunity to
obtain photometric measurements of Saturn's two inner medium-sized
satellites, Mimas and Enceladus. Telescopic observations of albedo
variegations on Mimas have never been obtained, while Enceladus was
previously observed by Franz and Millis (Icarus vol. 24, p. 433, 1975).
Voyager lightcurve observations of both satellites were obtained by
Buratti and Veverka (Icarus vol. 58, p. 254, 1984); good orbital coverage
was attained for Enceladus, but Mimas's coverage was limited to only
one hemisphere (90-270 degrees). Our telescopic observations of Mimas
are also somewhat limited (due to the similarity of Mimas's orbital
period to a terrestrial day), but we did obtain measurements at
longitudes not imaged by Voyager.

Voyager observations of Mimas (Buratti and Veverka, op. cit.) show
no significant albedo variegations on the satellite. Our preliminary
reductions, obtained by producing ratios of the brightness of Mimas
with Titan (which has a well-established lightcurve), confirm this view
and extend it to areas unseen by the spacecraft.

Our observations of Enceladus show that this satellite has albedo
variegations of at least 10% on its surface. Unlike Tethys, Dione, and
Rhea, Enceladus is brighter on the trailing side rather than the
leading side. This result is in agreement with both the Voyager
observations and the groundbased results of Franz and Millis. However,
the amplitude of our derived lightcurve is less than that obtained
by Franz and Millis.